Abstract
Abstract Here, we report on the unique observation of flaring coronal loops at the solar limb using high-resolution imaging spectropolarimetry from the Swedish 1 m Solar Telescope. The vantage position, orientation, and nature of the chromospheric material that filled the flare loops allowed us to determine their magnetic field with unprecedented accuracy using the weak-field approximation method. Our analysis reveals coronal magnetic field strengths as high as 350 G at heights up to 25 Mm above the solar limb. These measurements are substantially higher than a number of previous estimates and may have considerable implications for our current understanding of the extended solar atmosphere.
Highlights
The structure and dynamics of the most energetic events in the solar outer atmosphere such as flares, eruptions, coronal loops, and CMEs are controlled by the magnetic field
Our analysis reveals coronal magnetic field strengths as high as 350 G at heights up to 25 Mm above the solar limb
Footpoints of the observed flare loops were not detected in Swedish m Solar Telescope (SST) data, suggesting that they are behind the limb
Summary
The structure and dynamics of the most energetic events in the solar outer atmosphere such as flares, eruptions, coronal loops, and CMEs are controlled by the magnetic field. We report on the unique observations of the flaring coronal loops during this event at the solar limb using high-resolution imaging spectropolarimetry in the line of singly ionized calcium at 8542.1 Å, from the Swedish 1 m Solar Telescope. The CRISP data comprised of imaging spectropolarimetry in the Ca II 8542 Å line consisted of 21 line positions with an irregular step These positions were −1.75 Å to +1.75 Å (±1.75, ±0.945, ±0.735, ±0.595, ±0.455, ±0.35, ±0.28, ±0.21, ±0.14, ±0.07, 0.0 Å) from line core (see the animation associated with Figure 8(a) showing a full spectral scan).
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